2020A&A...641A.101B


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET21:15:52

2020A&A...641A.101B - Astronomy and Astrophysics, volume 641A, 101-101 (2020/9-1)

An underlying clock in the extreme flip-flop state transitions of the black hole transient Swift J1658.2-4242.

BOGENSBERGER D., PONTI G., JIN C., BELLONI T.M., PAN H., NANDRA K., RUSSELL T.D., MILLER-JONES J.C.A., MUNOZ-DARIAS T., VYNATHEYA P. and VINCENTELLI F.

Abstract (from CDS):


Aims. Flip-flops are top-hat-like X-ray flux variations, which have been observed in some transient accreting black hole binary systems, and feature simultaneous changes in the spectral hardness and the power density spectrum (PDS). They occur at a crucial time in the evolution of these systems, when the accretion disc emission starts to dominate over coronal emission. Flip-flops remain a poorly understood phenomenon, so we aim to thoroughly investigate them in a system featuring several such transitions.
Methods. Within the multitude of observations of Swift J1658.2-4242 during its outburst in early 2018, we detected 15 flip-flops, enabling a detailed analysis of their individual properties and the differences between them. We present observations by XMM-Newton, NuSTAR, Astrosat, Swift, Insight-HXMT, INTEGRAL, and ATCA. We analysed their light curves, searched for periodicities, computed their PDSs, and fitted their X-ray spectra, to investigate the source behaviour during flip-flop transitions and how the interval featuring flip-flops differs from the rest of the outburst.
Results. The flip-flops of Swift J1658.2-4242 are of an extreme variety, exhibiting flux differences of up to 77% within ∼100s, which is much larger than what has been seen previously. We observed radical changes in the PDS simultaneous with the sharp flux variations, featuring transitions between the quasi-periodic oscillation types C and A, which have never been observed before. Changes in the PDS are delayed, but more rapid than changes in the light curve. Flip-flops occur in two intervals within the outburst, separated by about two weeks in which these phenomena were not seen. Transitions between the two flip-flop states occurred at random integer multiples of a fundamental period of 2.761ks in the first interval and 2.61ks in the second. Spectral analysis reveals the high and low flux flip-flop states to be very similar, but distinct from intervals lacking flip-flops. A change of the inner temperature of the accretion disc is responsible for most of the flux difference in the flip-flops. We also highlight the importance of correcting for the influence of the dust scattering halo on the X-ray spectra.

Abstract Copyright: © D. Bogensberger et al. 2020

Journal keyword(s): accretion, accretion disks - black hole physics - X-rays: binaries - time

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* GU Mus HXB 11 26 26.5947467816 -68 40 32.888148788           K3V-K7V 675 1
2 MAXI J1535-571 XB* 15 35 19.73 -57 13 48.1           ~ 62 0
3 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1040 0
4 4U 1642-45 LXB 16 45 47.7 -45 36 40           ~ 383 1
5 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1727 1
6 SWIFT J1658.2-4242 X 16 58 12.64 -42 41 54.4           ~ 20 0
7 MAXI J1659-152 LXB 16 59 01.680 -15 15 28.73           ~ 194 0
8 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1791 0
9 PMN J1713-4257 Rad 17 13 48.16 -42 57 21.5           ~ 2 0
10 VCS4 J1717-3948 Rad 17 17 38.6013215 -39 48 52.668940           ~ 11 0
11 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 616 0
12 [KRL2007b] 312 LXB 18 17 43.537 -33 01 07.80           ~ 140 0
13 V* V406 Vul HXB 18 58 41.580 +22 39 29.40 15.00 15.65 15.31     G5V-K0V 324 0
14 Granat 1915+105 LXB 19 15 11.54938 +10 56 44.7585           ~ 2321 0
15 ICRF J193925.0-634245 Sy2 19 39 25.02671 -63 42 45.6255   18.87 18.37 17.64   ~ 975 1

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2020.11.28-21:15:52

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